Fig. REF  presents the maximum gravitational mass as a function both of the central energy density and the central baryon density. In particular, we present the results of 23 hadronic EoSs [1]}, for the non-rotating and maximally-rotating case, Tolman VII analytical solution, Eq. (REF ), data from Cook et al. [2]} and Salgado et al. [3]}, as well as the newly added data for the non-rotating and maximally-rotating case, both in \((v_{s}/c)^2=1/3\)  and \((v_{s}/c)^2=1\) , at the transition densities under consideration. Adopting the Eq. (REF ) for the range of the gravitational mass of the low mass component in the GW190814 event, the central energy density can be constrained in the range \(\varepsilon _{\rm c}/c^{2} = [2.53,2.89]~10^{15}~{\rm gr}~{\rm cm^{-3}}\) , meaning that neutron stars with higher values of central energy density cannot exist. Furthermore, from Fig. REF , we can also extract the corresponding region for the central baryon density, that is \(n_{c} = [7.27,8.09]~n_{s}\) . Finally, all the extracted EoSs meet the limit for the central energy/baryon density as they are included in the region described under Eq. (REF ).
